Analysis of Accelerated Particle Characteristics in Solar Explosions

Solar flares and coronal mass ejections (CMEs) are two major solar explosions, which are responsible for the production of solar energetic particles. These energetic particles are typically accelerated in the corona and then move downward to the chromosphere or upward to the interplanetary space. The downward motion of energetic particles is mainly flare-associated and can be investigated via imaging and spectral analysis. The energetic particles transport to/in the interplanetary space can come from a flare, a CME-driven shock, or an interplanetary shock, and are usually traced by radio dynamic spectrogram and in-situ measurements. Studying the non-thermal radiations in the solar atmosphere together with the interplanetary shocks will be helpful to diagnose the physical processes of particle acceleration and transport. In this project, we attempt to analyze the dynamics of non-thermal electrons during the transport in the solar atmosphere by combining the images from multiple wavelengths, as well as the hard X-ray and microwave spectra, with the theoretic trap-plus-precipitating model. Moreover, we attempt to investigate the acceleration efficiency of different types of shocks based on the in-situ solar wind and particle measurements and clarify the associated solar eruptive events by comparing with the coronagraph and EUV images. Therefore, this research work is an interdisciplinary study covering solar and interplanetary space. Our research results will provide the significant information on the issue of particle acceleration associated with solar explosions.